  In the context of low-viscosity protoplanetary discs (PPDs), the formation
scenarios of the Solar System should be revisited. In particular, the
Jupiter-Saturn pair has been shown to lock in the 2:1 mean motion resonance
while migrating generally inwards, making the Grand Tack scenario impossible.
We explore what resonant chains of multiple giant planets can form in a
low-viscosity disc, and whether these configurations can evolve into forming
the Solar System in the post gas disc phase. We used hydrodynamical simulations
to study the migration of the giant planets in a disc with viscosity
$\alpha=10^{-4}$. After a transition phase to a gas-less configuration, we
studied the stability of the obtained resonant chains through their
interactions with a disc of leftover planetesimals by performing N-body
simulations using rebound. The gaps open by giant planets are wider and deeper
for lower viscosity, reducing the damping effect of the disc and thus weakening
resonant chains. Exploring numerous configurations, we found five stable
resonant chains of four or five planets. In a thin PPD, the four giant planets
revert their migration and migrate outwards. After disc dispersal, under the
influence of a belt of planetesimals, some resonant chains undergo an
instability phase while others migrate smoothly over a billion years. For three
of our resonant chains, about 1% of the final configurations pass the four
criteria to fit the Solar System. The most successful runs are obtained for
systems formed in a cold PPD with a massive planetesimal disc. This work
provides a fully consistent study of the dynamical history of the Solar
System's giant planets, from the protoplanetary disc phase up to the giant
planet instability. Although building resonant configurations is difficult in
low-viscosity discs, we find it possible to reproduce the Solar System from a
cold, low-viscosity protoplanetary disc.
