The peak of galactic star formation occurs between redshifts 1 to 3. Star-forming galaxies at these redshifts are shown to have irregular morphologies, at ultraviolet wavelengths, dominated by massive star-forming regions, typically called 'clumps'. Whilst these clumps have been numerously observed with star formation tracers, the molecular gas that fuels star-formation has remained elusive - outside of a couple of cases of gravitational lensing at redshift ~1. I will present a sample of galaxies from redshift 1 to 4.5 and show their morphologies in molecular gas tracers - with the focus of looking for clumps. Of particular focus, will be what has been dubbed the typical star forming galaxy at cosmic noon; BX610. By creating and subtracting a kinematic model we have been able to identify multiple clumps in CO(4-3) that are not otherwise visible in the map of the CO line emission. From these identified clumps we identify two categories of clump. Those which appear to be isolated and show no overlap with observations in other tracers. Secondly, those which show a partial overlap with previous rest frame UV/optical HST observations. We will discuss the cause of this offset between the two tracers, with a focus on the fact that star formation may be occurring at different rates across these clumps. Using the sample, we will also present the conditions for the formation of molecular gas clumps in these galaxies.