Within multi-planet systems observed by the Kepler mission, a trend has been discovered correlating the sizes of adjacent planets and orbital period ratios of adjacent planet pairs within the same system. I analyze how this “peas-in-a-pod” architecture manifests in simulated super-Earth exoplanet systems governed by different pebble/planetesimal accretion models that vary in limiting embryo isolation mass. I aim to identify discontinuities that arise in these architectures and their implications for each formation model.