  Many features of the outer solar system are replicated in numerical
simulations if the giant planets undergo an orbital instability that ejects one
or more ice giants. During this instability, Jupiter and Saturn's orbits
diverge, crossing their 2:1 mean motion resonance (MMR), and this
resonance-crossing can excite the terrestrial planet orbits. Using a large
ensemble of simulations of this giant planet instability, we directly model the
evolution of the terrestrial planet orbits during this process, paying special
attention to systems that reproduce the basic features of the outer planets. In
systems that retain four giant planets and finish with Jupiter and Saturn
beyond their 2:1 MMR, we find at least an 85% probability that at least one
terrestrial planet is lost. Moreover, systems that manage to retain all four
terrestrial planets often finish with terrestrial planet eccentricities and
inclinations larger than the observed ones. There is less than a ~5% chance
that the terrestrial planet orbits will have a level of excitation comparable
to the observed orbits. If we factor in the probability that the outer
planetary orbits are well-replicated, we find a probability of 1% or less that
the orbital architectures of the inner and outer planets are simultaneously
reproduced in the same system. These small probabilities raise the prospect
that the giant planet instability occurred before the terrestrial planets had
formed. This scenario implies that the giant planet instability is not the
source of the Late Heavy Bombardment and that terrestrial planet formation
finished with the giant planets in their modern configuration.
