  Advances in computing power and numerical methodologies over the past several
decades sparked a prolific output of dynamical investigations of the late
stages of terrestrial planet formation. Among other peculiar inner solar system
qualities, the ability of simulations to reproduce the small mass of Mars
within the planets' geochemically inferred accretion timescale of <10 Myr after
the appearance of calcium aluminum-rich inclusions (CAIs) is arguably
considered the gold standard for judging evolutionary hypotheses. At present, a
number of independent models are capable of consistently generating Mars-like
planets and simultaneously satisfying various important observational and
geochemical constraints. However, all models must still account for the effects
of the epoch of giant planet migration and orbital instability; an event which
dynamical and cosmochemical constraints indicate occurred within the first 100
Myr after nebular gas dispersal. If the instability occurred in the first few
Myr of this window, the disturbance might have affected the bulk of Mars'
growth. In this manuscript, we turn our attention to a scenario where the
instability took place after t=50 Myr. Specifically, we simulate the
instability's effects on three nearly-assembled terrestrial systems that were
generated via previous embryo accretion models and contain three large
proto-planets with orbits interior to a collection of ~Mars-mass embryos and
debris. While the instability consistently triggers a Moon-forming impact and
efficiently removes excessive material from the Mars-region in our models, we
find that our final systems are too dynamically excited and devoid of Mars and
Mercury analogs. Thus, we conclude that, while possible, our scenario is far
more improbable than one where the instability either occurred earlier, or at a
time where Earth and Venus' orbits were far less dynamically excited.
