  Super-Earths within the same close-in, compact planetary system tend to
exhibit a striking degree of uniformity in their radius, mass, and orbital
spacing, and this 'peas-in-a-pod' phenomenon itself serves to provide one of
the strongest constrains on planet formation at large. While it has been
recently demonstrated from independent samples that such planetary uniformity
occurs for both configurations near and distant from mean motion resonance, the
question thus remains if the strength of this uniformity itself differs between
near-resonant and nonresonant configurations such that the two modes may be
astrophysically distinct in their evolution. We thus provide in this work a
novel comparative size uniformity analysis for 48 near-resonant and 251
nonresonant multi-planet systems from the California Kepler Survey catalog,
evaluating uniformity both across systems and between planetary pairs within
the same system. We find that while multiplanet configurations exhibit strong
peas-in-a-pod size uniformity regardless of their proximity to resonance,
near-resonant configurations display enhanced intra-system size uniformity as
compared to their analogous nonresonant counterparts at the level of both
entire systems and subsystem planetary pairs and chains. These results are
broadly consistent with a variety of formation paradigms for multiplanet
systems, such as convergent migration within a turbulent protoplanetary disk or
planet-planet interactions incited by postnebular dynamical instabilities.
Nevertheless, further investigation is necessary to ascertain whether the
nonresonant and near-resonant planetary configurations respectively evolve via
a singular process or mechanisms that are dynamically distinct.
