Stellar density maps of our red giants in the three metallicity bins described in the text with metal poor in the leftmost panel and metal rich in the right. The general evolution in morphology is a decrease in the outer substructure in both Clouds with increasing stellar metallicity. The most metal-rich bin shows the LMC and SMC to be isolated, whereas the metal-poor bin shows the Clouds to be connected, both in the Magellanic Bridge region and further south where the outer stellar arc of the LMC attaches to the eastern edge of the SMC. The most metal-poor giants in the SMC show a high central density, with the outer regions appearing stretched horizontally, likely due to tidal interactions with the LMC. At the metal-rich end, the SMC is much more compact and shows a weaker signature of tidal disruption.