Planet radii as a function of their semi-major axis for all three models after 3 Gyr of evolution. The color of each point indicates the atmosphere mass fraction. The dashed lines show the core radius at the pebble isolation mass at the start and end of the disc lifetime for a planet with a density of 3.6 g/cm³, which is a typical density for our planets. In all models, planets above pebble isolation mass that orbit farther away from the star are smaller as their contraction rate is faster. When varying the inner edge, planets farther away from the star are able to reach radii as low as ~2 R_⊕. However, planets that accrete a massive enough atmosphere (~10% of core mass) remain large resist contraction.