Modern galaxy formation simulations routinely reach the scales necessary to self-consistently capture the internal structure of molecular clouds while simultaneously accounting for galactic-scale gas flows. Furthermore, individual stars can be treated as resolved objects, even in cosmological environments. I will present such a suite of simulated dwarf galaxies, in which I systematically explore the impact of both internal (e.g., assumptions about stellar evolution) and external (e.g., growth history) factors. Finally, with individual stars directly accessible in our simulations, we can derive observables in a self-consistent manner. I will show how this approach can help guide next-generation observatories and further constrain galaxy formation theory.
