  To reproduce the orbits and masses of the terrestrial planets (analogs) of
the solar system, most studies scrutinize simulations for success as a batch.
However, there is insufficient discussion in the literature on the likelihood
of forming planet analogs simultaneously in the same system (analog system). To
address this issue, we performed 540 N-body simulations of protoplanetary disks
representative of typical models in the literature. We identified a total of
194 analog systems containing at least three analogs, but only 17 systems
simultaneously contained analogs of the four terrestrial planets. From an
analysis of our analog systems, we found that, compared to the real planets,
truncated disks based on typical outcomes of the Grand Tack model produced
analogs of Mercury and Mars that were too dynamically cold and located too
close to the Venus and Earth analogs. Additionally, all the Mercury analogs
were too massive, while most of the Mars analogs were more massive than Mars.
Furthermore, the timing of the Moon-forming impact was too early in these
systems, and the amount of additional mass accreted after the event was too
great. Therefore, such truncated disks cannot explain the formation of the
terrestrial planets. Our results suggest that forming the four terrestrial
planets requires disks with the following properties: 1) Mass concentrated in
narrow core regions between ~0.7-0.9 and ~1.0-1.2 au; 2) an inner region
component starting at ~0.3-0.4 au; 3) a less massive component beginning at
~1.0-1.2 au; 4) embryos rather than planetesimals carrying most of the disk
mass; and 5) Jupiter and Saturn placed on eccentric orbits.
