  The formation history of Jupiter has been of interest due to its ability to
shape the solar system's history. Yet little attention has been paid to the
formation and growth of Saturn and the other giant planets. Here, we explore
the implications of the simplest disc and pebble accretion model with
steady-state accretion on the formation of giant planets in the solar system
through N-body simulations. We conducted a statistical survey of different disc
parameters and initial conditions of the protoplanetary disc to establish which
combination best reproduces the present outer solar system. We examined the
effect of the initial planetesimal disc mass, the number of planetesimals and
their size-frequency distribution slope, pebble accretion prescription, and
sticking efficiency on the likelihood of forming gas giants and their orbital
distribution. The results reveal that the accretion sticking efficiency is the
most sensitive parameter for controlling the final masses and number of giant
planets. We have been unable to replicate the formation of all three types of
giant planets in the solar system in a single simulation. The probability
distribution of the final location of the giant planets is approximately
constant in $\log r$, suggesting there is a slight preference for formation
closer to the Sun but no preference for more massive planets to form closer.
The eccentricity distribution has a higher mean for more massive planets,
indicating that systems with more massive planets are more violent. The
formation timescales of the cores of the gas giants are distinct, suggesting
that they formed sequentially.
