  Orbital evolution is a critical process that sculpts planetary systems,
particularly during their early stages where planet-disk interactions are
expected to lead to the formation of resonant chains. Despite the theoretically
expected prominence of such configurations, they are scarcely observed among
long-period giant exoplanets. This disparity suggests an evolutionary sequence
wherein giant planet systems originate in compact multiresonant configurations,
but subsequently become unstable, eventually relaxing to wider orbits--a
phenomenon mirrored in our own solar system's early history. In this work, we
present a suite of N-body simulations that model the instability-driven
evolution of giant planet systems, originating from resonant initial
conditions, through phases of disk dispersal and beyond. By comparing the
period ratio and normalized angular momentum distributions of our synthetic
aggregate of systems with the observational census of long-period Jovian
planets, we derive constraints on the expected rate of orbital migration, the
efficiency of gas-driven eccentricity damping, and typical initial
multiplicity. Our findings reveal a distinct inclination toward densely packed
initial conditions, weak damping, and high giant planet multiplicities.
Furthermore, our models indicate that resonant chain origins do not facilitate
the formation of Hot Jupiters via the coplanar high-eccentricity pathway at
rates high enough to explain their observed prevalence.
