Abstract: On large scales the Universe is well described by a cosmological model where matter primarily comprises cold dark matter (CDM), a single collision-less particle species with negligible primordial thermal dispersion. On galactic scales, numerical CDM-only simulations predict identical rotation curves for fixed dark matter halo mass. However, observed dwarf galaxies exhibit diverse rotation curves. The addition of galaxy formation (baryonic) physics in which star formation and subsequent feedback rearrange central dark matter densities has been proposed as a solution to the diversity of rotation curves problem, though previous CDM simulations with baryons have struggled to simultaneously reproduce the most steeply and slowly rising rotation curves, and compact and extended galaxies at fixed stellar mass. An alternative solution is dark matter self-interactions which collisionally thermalize dark matter particles and alter central halo densities. In this seminar, I will discuss a new suite of high-resolution hydrodynamical cosmological zoom-in simulations aimed to cohesively explore dwarf galaxy diversity in CDM with baryons and multiple models of self-interacting dark matter with and without baryons. We find the CDM and low cross-section SIDM simulations with baryons both produce steeply and slowly rising rotation curves that are connected to their host galaxies' surface brightness, like observed galaxies. This prompts us to explore additional galaxy properties which may distinguish the two DM models.