In this work, we choose the δ-Scuti KOI-976 - KIC 3441784 - as our target system for analysis. The Exoplanet Follow-up Observing Program (ExoFOP) lists this system as an eclipsing binary consisting of an F0 star and an M-dwarf companion. The F0 star (hereafter called the primary star) is rotating rapidly with an ExoFOP-reported v sin(i) of 120 km/s and seismically induced amplitude variations of ~3.0 mmag. This work includes a four-stage analysis of KOI-976, observed by Kepler. We first measure the primary star's obliquity angle and rotation rate by applying asteroseismic theory to KOI-976's seismically active out-of-transit photometry. We then subtract out stellar variability from KOI-976's short-cadence transit event to prepare the data set for further analysis. Finally, we perform a joint analysis of both the long-cadence and short-cadence Kepler transit light curves using a gravity-darkened model to measure bulk parameters of the system and to test the validity of variability subtraction as a path for cleaning transit light curves.(1 data file).