The Magellanic System is the epitome of gas-rich, interacting dwarf systems. Their proximity, low-metallicity and richness in hydrogen, the primary constituent for formation of stars, makes them the perfect target for high-resolution and high sensitivity observations of the un-enriched ISM. Providing ~10 pc resolutions, we are able to examine the morphological characteristics, distribution, and kinematical properties of the ISM at scales unavailable any where else. We are part way through a larger-scale survey to observe the CO(J=1-0) transition throughout the Magellanic System. We show that the small and weak CO clouds are, in fact, much smaller and less massive than previously understood, particularly in the SMC, indicating a poorly-enriched, un-evolved ISM. We also show to high resolution, a puzzlingly poor detailed correlation of the CO and HI fractions in the ISM. For the first time, we resolve multi-component CO profiles in the SMC, indicative of some recent major energetic perturbing events in the body of the SMC.