  The characterization of Super-Earth-to-Neptune sized exoplanets relies
heavily on our understanding of their formation and evolution. In this study,
we link a model of planet formation by pebble accretion to the planets'
long-term observational properties by calculating the interior evolution,
starting from the dissipation of the protoplanetary disk. We investigate the
evolution of the interior structure in 5-20 Earth masses planets, accounting
for silicate redistribution caused by convective mixing, rainout (condensation
and settling), and mass loss. Specifically, we have followed the fate of the
hot silicate vapor that remained in the planet's envelope after planet
formation, as the planet cools. We find that disk dissipation is followed by a
rapid contraction of the envelope within 10 Myr. Subsequent cooling leads to
substantial growth of the planetary core through silicate rainout, accompanied
by inflated radii, in comparison to the standard models of planets that formed
with core-envelope structure. We examine the dependence of rainout on the
planet's envelope mass, distance from its host star, its silicate mass, and the
atmospheric opacity. We find that the population of planets formed with
polluted envelopes can be roughly divided in three groups, based on the mass of
their gas envelopes: bare rocky cores that have shed their envelopes,
super-Earth planets with a core-envelope structure, and Neptune-like planets
with diluted cores that undergo gradual rainout. For polluted planets formed
with envelope masses below 0.4 Earth mass, we anticipate that the inflation of
the planet's radius caused by rainout will enhance mass loss by a factor of 2-8
compared to planets with non-polluted envelopes. Our model provides an
explanation for bridging the gap between the predicted composition gradients in
massive planets and the core-envelope structure in smaller planets.
