Star formation is an important physical observable that traces the complex processes involved in galaxy evolution. The inflows and outflows of gas that drive star formation and quenching as well as the timescales upon which they act are still not well understood. We select 12 galaxies from the UVCANDELS survey where a total of 10 HST bands including UV follow up in F275W allow for us to reconstruct the star formation histories of multiple regions across each galaxy. We create spatially resolved maps of the galaxy regions colored by stellar mass, SFR, and sSFR to identify where and when stars are actively forming. We then reproduce the resolved star forming main sequence (rSFMS) for each galaxy at the time of observation and 1 Gyr lookback time noting the slope, scatter, and normalization for each. We compare offsets for each galaxy's slope, scatter, and normalization from the global trend. This allows us to explore how galaxies transition between clumpy and smooth star formation patterns and how these transitions are linked to a galaxy's stellar mass and SFR. Comparing the rSFMS with trends in the property maps we can infer the timing and location of bursts of star formation and better understand the connection between star formation and the ISM.