V1178 Tau is a double-lined spectroscopic eclipsing binary in NGC1817, one of the more massive open star clusters observed during the K2 mission. We have determined the orbital period (P = 2.08595d) for the first time, and we model radial velocity measurements from the HARPS and ALFOSC spectrographs, light curves collected by Kepler, and ground based light curves using the Eclipsing Light Curve code (ELC; Orosz & Hauschildt 2000). The modeling of V1178 Tau has provided evidence of a possible third object in the system. With an age of approximately a billion years and a short orbital period, V1178 Tau’s orbit is not circularized as one would expect but is significantly eccentric. Further evidence for a potential third light can also be seen in the broadening functions used to obtain the radial velocities. After attempting to account for the potential presence of a third body, we present masses and radii for the stars in the binary, allowing for a reddening-independent means of determining the cluster age. V1178 Tau is particularly useful for calculating the age of the cluster because one of the stars in the system is close to the cluster turnoff, providing a precise age determination. Furthermore, because one of the stars in the binary is a δ Scuti variable, further analysis will give insight into their pulsations.