  Population synthesis models of planetary systems developed during the last
$\sim$15 years could reproduce several of the observables of the exoplanet
population, and also allowed to constrain planetary formation models. We
present our planet formation model, which calculates the evolution of a
planetary system during the gaseous phase. The code incorporates relevant
physical phenomena for the formation of a planetary system, like
photoevaporation, planet migration, gas accretion, water delivery in embryos
and planetesimals, a detailed study of the orbital evolution of the
planetesimal population, and the treatment of the fusion between embryos,
considering their atmospheres. The main goal of this work, unlike other works
of planetary population synthesis, is to find suitable scenarios and physical
parameters of the disc to form solar system analogs. We are specially
interested in the final planet distributions, and in the final surface density,
eccentricity and inclination profiles for the planetesimal population. These
final distributions will be used as initial conditions for N-body simulations,
to study the post-oligarchic formation in a second work. We then consider
different formation scenarios, with different planetesimal sizes and different
type I migration rates. We find that solar system analogs are favored in
massive discs, with low type I migration rates, and small planetesimal sizes.
Besides, those rocky planets within their habitables zones are dry when discs
dissipate. At last, the final configurations of solar system analogs include
information about the mass and semimajor-axis of the planets, water contents,
and the properties of the planetesimal remnants.
