  This work is the second part of a project that attempts to analyze the
formation of Solar system analogues (SSAs) from the gaseous to the post-gas
phase, in a self-consistently way. In the first paper (PI) we presented our
model of planet formation during the gaseous phase which provided us with
embryo distributions, planetesimal surface density, eccentricity and
inclination profiles of SSAs, considering different planetesimal sizes and type
I migration rates at the time the gas dissipates. In this second work we focus
on the late accretion stage of SSAs using the results obtained in PI as initial
conditions to carry out N-body simulations. One of our interests is to analyze
the formation of rocky planets and their final water contents within the
habitable zone. Our results show that the formation of potentially habitable
planets (PHPs) seems to be a common process in this kind of scenarios. However,
the efficiency in forming PHPs is directly related to the size of the
planetesimals. The smaller the planetesimals, the greater the efficiency in
forming PHPs. We also analyze the sensitivity of our results to scenarios with
type I migration rates and gap-opening giants, finding that both phenomena act
in a similar way. These effects seem to favor the formation of PHPs for small
planetesimal scenarios and to be detrimental for scenarios formed from big
planetesimals. Finally, another interesting result is that the formation of
water-rich PHPs seems to be more common than the formation of dry PHPs.
