  The formation of the solar system's terrestrial planets has been numerically
modeled in various works, and many other studies have been devoted to
characterizing our modern planets' chaotic dynamical state. However, it is
still not known whether our planet's fragile chaotic state is an expected
outcome of terrestrial planet accretion. We use a suite of numerical
simulations to present a detailed analysis and characterization of the
dynamical chaos in 145 different systems produced via terrestrial planet
formation in Kaib and Cowan (2015). These systems were created in the presence
of a fully formed Jupiter and Saturn, using a variety of different initial
conditions. They are not meant to provide a detailed replication of the actual
present solar system, but rather serve as a sample of similar systems for
comparison and analysis. We find that dynamical chaos is prevalent in roughly
half of the systems we form. We show that this chaos disappears in the majority
of such systems when Jupiter is removed, implying that the largest source of
chaos is perturbations from Jupiter. Chaos is most prevalent in systems that
form 4 or 5 terrestrial planets. Additionally, an eccentric Jupiter and Saturn
is shown to enhance the prevalence of chaos in systems. Furthermore, systems in
our sample with a center of mass highly concentrated between 0.8 -1.2 AU
generally prove to be less chaotic than systems with more exotic mass
distributions. Through the process of evolving systems to the current epoch, we
show that late instabilities are quite common in our systems. Of greatest
interest, many of the sources of chaos observed in our own solar system (such
as the secularly driven chaos between Mercury and Jupiter) are shown to be
common outcomes of terrestrial planetary formation.
