In this talk we will discuss results regarding the gas phase structure and [C II] 158 μm emission in sub-pc resolution simulations of a self-regulated ISM. We explore the metallicity dependence of the relation between [C II] luminosity and star formation rate, showing that the scatter in the observed relation in local dwarf galaxies could be driven by metallicity. In addition, we will discuss the importance of magnetic fields and the effects of varying gas surface density on the ISM phase structure. Finally, we will apply the theory of Pressure-Regulated Feedback-Modulated star formation to our simulations.