  The Jupiter-Saturn chaotic excitation (JSCE) scenario proposes that the
protoplanetary disk was dynamically excited and depleted beyond ~1-1.5 au in a
few Myr, offering a new and plausible explanation for several observed
properties of the inner solar system. Here, we expanded our previous work by
conducting a comprehensive analysis of 37 optimal terrestrial planet systems
obtained in the context of the JSCE scenario. Each optimal system harbored
exactly four terrestrial planets analogs to Mercury, Venus, Earth, and Mars. We
further investigated water delivery, feeding zones, and accretion history for
the planet analogs, which allowed us to better constrain the water distribution
in the disk. The main findings of this work are as follows: 1) the formation of
four terrestrial planets with orbits and masses similar to those observed in
our solar system in most of our sample, as evidenced by the dynamically colder
and hotter orbits of Venus-Earth and Mercury-Mars analogs, and the high success
rates of similar mutual orbital separations (~40-85%) and mass ratios of the
planets (~70-90%) among the 37 systems; and 2) water was delivered to all
terrestrial planets during their formation through the accretion of
water-bearing disk objects from beyond ~1-1.5 au. The achievement of Earth's
estimated bulk water content required the disk to contain sufficient water mass
distributed within those objects initially. This requirement implies that
Mercury, Venus, and Mars acquired water similar to the amount on Earth during
their formation. Several of our planet analogs also matched additional
constraints, such as the timing of Moon formation by a giant impact, Earth's
late accretion mass and composition, and Mars's formation timescale.
