If you are content with a scale level of 1 (or even less if possible) you can make your planet as large or small, as near to or as far from its star, and give it any climate and any surface conditions, you may desie for your story.

For example, a world with 1.7 times the radius or 1.7 times the diameter of earth would have a surface area 2.89 times that of Earth and a volume 4.912867 that of Earth. If it had the same overall ensity it would have 4.912867 times the mass of Earth, but of course the overall density of planets can vary.

Dole had a formula for how he believed the mass of world would chancege its density and htus its volume. So on page 53 Dole wrote that a planet with a surface gravity of 1.5 g would have a mass of 2.35 Earth mass, a radius of 1.25 Earth radius, and an escape velocity of 15.3 kilometers per second. A mass of 2.35 Earth mass would be just a bit less than 2.4 Earth mass, while a radius of 1.25 Earth radius gives a surface area 1.56 that of Earth and a 1.952972 volume that of Earth.

On the minimum size, Dole decided on page 54 that a planet with ane scape velocity of 6.25 kilometers per second might be able to retain an oxygen atmosphere for geological eras of time. That corresponds to mass 0.195 of Earth, a radius of 0.63 Earth radius, and a surface gravity of 0.49 G. But Dole thought that such a small planet would not be able to form an oxygen rich atmosphere, and onpage 57decided tha the smallest planet that could form an oxygen rich atmosphere might have about 0.4 the mass of Earth, a radisu 0.78 that of Earth, and a surface gravity of 0.68 g.

In recent decades, many scientists have considered the requirements for a world to be habitable. Unlike Dole, they seem to have concentrated on the more general case of worlds habitable for liquid water using lifeforms in general, instead of the more limited case of worlds habitable for humans (or for beings with similar environmental requiremetns) in particular. Of course most science fiction writers are interested in the more restricted definition of habitability.

One modern discussion of the mass range of a habitable world is in Heller and Barnes "Exomoon habitabilty constrained by illumination and tidal heating", 2013, pages 3 to 4:

A minimum mass of an exomoon is required to drive a magnetic shield on a billion-year timescale (Ms ≳ 0.1M⊕, Tachinami et al. 2011); to sustain a substantial, long-lived atmosphere (Ms ≳ 0.12M⊕, Williams et al. 1997; Kaltenegger 2000); and to drive tectonic activity (Ms ≳ 0.23M⊕, Williams et al. 1997), which is necessary to maintain plate tectonics and to support the carbon-silicate cycle. Weak internal dynamos have been detected in Mercury and Ganymede (Kivelson et al. 1996; Gurnett et al. 1996), suggesting that satellite masses > 0.25M⊕ will be adequate for considerations of exomoon habitability. This lower limit, however, is not a fixed number. Further sources of energy – such as radiogenic and tidal Heller & Barnes (2013) – Exomoon habitability constrained by illumination and tidal heating, and the effect of a moon’s composition and structure – can alter our limit in either direction. An upper mass limit is given by the fact that increasing mass leads to high pressures in the moon’s interior, which will increase the mantle viscosity and depress heat transfer throughout the mantle as well as in the core. Above a critical mass, the dynamo is strongly suppressed and becomes too weak to generate a magnetic field or sustain plate tectonics. This maximum mass can be placed around 2M⊕ (Gaidos et al. 2010; Noack & Breuer 2011; Stamenković et al. 2011). Summing up these conditions, we expect approximately Earth-mass moons to be habitable, and these objects could be detectable with the newly started Hunt for Exomoons with Kepler (HEK) project (Kipping et al. 2012).

So their sources indicate minium masses for habitable worlds of 0.1 Earth, or 0.12 Earth, or 0.23 Earth, and a maximum mass for habitable worlds of about 2.0 Earth mass.

I note that with similar average density, a world with about 2.0 Earth maass would have less mass than Dole's upper limit. Dole's upper limit had 2.35 Earth mass, 1.25the radius, of Earth, an escape velocity of 15.3 kilometers per second, and a surfacegravity of 1.5 g. A world that has 2.0 Earht mas sor less would have less of all those factors.

Low mass worlds will have low escape velocities and rapidly lose their atmospheres as gases escape into outer space. The paper studies low mass water worlds entirely covered by very deep oceans of water, with wiht atmospherees purely of water vapor. I note that worlds with such vast oceans would have a lot of liquid and so could replace water vapor escaping into space with evaporated surface water for very long periods of time.

And there is one clase of water worlds which could have evenless mass than the ones discussed in that paper. Water worlds which retain their liquid water with solid lids on top of it. Those worlds would have vast world wide oceans many kilometers deep underneath planet wide ice sheets many kilometers deep.

Of those worlds with internal oceans, the samllest is Saturn's moon Enceladus, 513.2 by 502.8 by 496.6 kilometers. Encledaus has a mass of about 1.080 times 10 to the 20th power kilograms, or 0.00018 the mass of Earth, which is much smaller than the minimum mass of 0.268 Earth mass for water worlds without natural roofs all over them.

Planets more masive than Earth, but less massive than ice giants, are called super Earths. Super Earths may water planets, palnets totally covered with water.

This is consiereable scientific discussion about the possibilities that super Earths, including thsoe wich are water worlds, are habitable. As mentioned above, it has been claimed that worlds with more than 2 times the mass of Earth would not have liquid metal cores and magnetic fields and plate tectonics.

This article mentins a study whichindictes that super Earths with four to six time sthe mas sof Earth would have the longest lasting metallic cores. And thus they should probably have magnetic fields and plate tectonics.

Here is a link to an article which claimes that A) large moons are necessary for habitablity, and 2) that super Earths are unlikely to form large moons.

If you are content with a scale level of 1 (or even less if possible) you can make your planet as large or small, as near to or as far from its star, and give it any climate and any surface conditions, you may desire for your story.

For example, a world with 1.7 times the radius or 1.7 times the diameter of Earth would have a surface area 2.89 times that of Earth and a volume 4.912867 that of Earth. If it had the same overall density it would have 4.912867 times the mass of Earth, but of course the overall density of planets can vary.

Dole had a formula for how he believed the mass of world would change its density and thus its volume. So on page 53 Dole wrote that a planet with a surface gravity of 1.5 g would have a mass of 2.35 Earth mass, a radius of 1.25 Earth radius, and an escape velocity of 15.3 kilometers per second. A mass of 2.35 Earth mass would be just a bit less than 2.4 Earth mass, while a radius of 1.25 Earth radius gives a surface area 1.56 that of Earth and a 1.952972 volume that of Earth.

On the minimum size, Dole decided on page 54 that a planet with an escape velocity of 6.25 kilometers per second might be able to retain an oxygen atmosphere for geological eras of time. That corresponds to mass 0.195 of Earth, a radius of 0.63 Earth radius, and a surface gravity of 0.49 g. But Dole thought that such a small planet would not be able to form an oxygen rich atmosphere, and on page 57 decided that the smallest planet that could form an oxygen rich atmosphere might have about 0.4 the mass of Earth, a radius 0.78 that of Earth, and a surface gravity of 0.68 g.

In recent decades, many scientists have considered the requirements for a world to be habitable. Unlike Dole, they seem to have concentrated on the more general case of worlds habitable for liquid water using lifeforms in general, instead of the more limited case of worlds habitable for humans (or for beings with similar environmental requirements) in particular. Of course most science fiction writers are interested in the more restricted definition of habitability.

One modern discussion of the mass range of a habitable world is in Heller and Barnes "Exomoon habitability constrained by illumination and tidal heating", 2013, pages 3 to 4:

A minimum mass of an exomoon is required to drive a magnetic shield on a billion-year timescale (Ms ≳ 0.1M⊕, Tachinami et al. 2011); to sustain a substantial, long-lived atmosphere (Ms ≳ 0.12M⊕, Williams et al. 1997; Kaltenegger 2000); and to drive tectonic activity (Ms ≳ 0.23M⊕, Williams et al. 1997), which is necessary to maintain plate tectonics and to support the carbon-silicate cycle. Weak internal dynamos have been detected in Mercury and Ganymede (Kivelson et al. 1996; Gurnett et al. 1996), suggesting that satellite masses > 0.25M⊕ will be adequate for considerations of exomoon habitability. This lower limit, however, is not a fixed number. Further sources of energy – such as radiogenic and tidal Heller & Barnes (2013) – Exomoon habitability constrained by illumination and tidal heating, and the effect of a moon’s composition and structure – can alter our limit in either direction. An upper mass limit is given by the fact that increasing mass leads to high pressures in the moon’s interior, which will increase the mantle viscosity and depress heat transfer throughout the mantle as well as in the core. Above a critical mass, the dynamo is strongly suppressed and becomes too weak to generate a magnetic field or sustain plate tectonics. This maximum mass can be placed around 2M⊕ (Gaidos et al. 2010; Noack & Breuer 2011; Stamenković et al. 2011). Summing up these conditions, we expect approximately Earth-mass moons to be habitable, and these objects could be detectable with the newly started Hunt for Exomoons with Kepler (HEK) project (Kipping et al. 2012).

So their sources indicate minimum masses for habitable worlds of 0.1 Earth, or 0.12 Earth, or 0.23 Earth, and a maximum mass for habitable worlds of about 2.0 Earth mass.

I note that with similar average density, a world with about 2.0 Earth mass would have less mass than Dole's upper limit. Dole's upper limit had 2.35 Earth mass, 1.25 the radius, of Earth, an escape velocity of 15.3 kilometers per second, and a surface gravity of 1.5 g. A world that has 2.0 Earth mass or less would have less of all those factors.

Low mass worlds will have low escape velocities and rapidly lose their atmospheres as gases escape into outer space. The paper studies low mass water worlds entirely covered by very deep oceans of water, with with atmospheres purely of water vapor. I note that worlds with such vast oceans would have a lot of liquid and so could replace water vapor escaping into space with evaporated surface water for very long periods of time.

And there is one class of water worlds which could have even less mass than the ones discussed in that paper. Water worlds which retain their liquid water with solid lids on top of it. Those worlds would have vast world wide oceans many kilometers deep underneath planet wide ice sheets many kilometers deep.

Of those worlds with internal oceans, the smallest is Saturn's moon Enceladus, 513.2 by 502.8 by 496.6 kilometers. Encledaus has a mass of about 1.080 times 10 to the 20^th power kilograms, or 0.00018 the mass of Earth, which is much smaller than the minimum mass of 0.268 Earth mass for water worlds without natural roofs all over them.

Planets more massive than Earth, but less massive than ice giants, are called super Earths. Super Earths may water planets, planets totally covered with water.

This is considerable scientific discussion about the possibilities that super Earths, including those which are water worlds, are habitable. As mentioned above, it has been claimed that worlds with more than 2 times the mass of Earth would not have liquid metal cores and magnetic fields and plate tectonics.

This article mentions a study which indicates that super Earths with four to six times the mass of Earth would have the longest lasting metallic cores. And thus they should probably have magnetic fields and plate tectonics.

Here is a link to an article which claims that A) large moons are necessary for habitability, and 2) that super Earths are unlikely to form large moons.