  The inner solar system's modern orbital architecture provides inferences into
the epoch of terrestrial planet formation; a ~100 Myr time period of planet
growth via collisions with planetesimals and other proto-planets. While classic
numerical simulations of this scenario adequately reproduced the correct number
of terrestrial worlds, their semi-major axes and approximate formation
timescales, they struggled to replicate the Earth-Mars and Venus-Mercury mass
ratios. In a series of past independent investigations, we demonstrated that
Mars' mass is possibly the result of Jupiter and Saturn's early orbital
evolution, while Mercury's diminutive size might be the consequence of a
primordial mass deficit in the region. Here, we combine these ideas in a single
modeled scenario designed to simultaneously reproduce the formation of all four
terrestrial planets and the modern orbits of the giant planets in broad
strokes. By evaluating our Mercury analogs' core mass fractions, masses, and
orbital offsets from Venus, we favor a scenario where Mercury forms through a
series of violent erosive collisions between a number of ~Mercury-mass embryos
in the inner part of the terrestrial disk. We also compare cases where the gas
giants begin the simulation locked in a compact 3:2 resonant configuration to a
more relaxed 2:1 orientation and find the former to be more successful. In 2:1
cases, the entire Mercury-forming region is often depleted due to strong
sweeping secular resonances that also tend to overly excite the orbits of Earth
and Venus as they grow. While our model is quite successful at replicating
Mercury's massive core and dynamically isolated orbit, the planets' low mass
remains extremely challenging to match. Finally, we discuss the merits and
drawbacks of alternative evolutionary scenarios and initial disk conditions.
