We analyze the kinematics as a function of stellar age for Andromeda (M31) mass analogs from the Illustris and Illustris TNG cosmological simulations. We divide the star particles into four age groups: < 1 Gyr, 1-5 Gyr, 5-10 Gyr, and >10 Gyr, and we compare the kinematics of these groups to that of the neutral gas cells. We calculate rotation curves for the stellar and gaseous components of each analog from 2 kpc to 20 kpc from the center of mass. We find that the lag, or asymmetric drift (AD), between the gas rotation curve and the stellar rotation curve on average increases with stellar age. This finding is consistent with observational measurements of AD in the disk of the Andromeda galaxy. When the M31 analogs are separated into groups based on merger history, we find that there is a difference in the AD of the analogs in the subgroup that corresponds to having had a 4:1 merger in a given time range compared to analogs that have not experienced a 4:1 merger in the same time frame. These differences are the most significant for recent 4:1 merger events (< 4 Gyr ago) and are therefore most visible in the 1-5 Gyr stellar age group where we find a difference in AD as large as 55 km/s. This subset of analogs that have had a 4:1 merger within the last 4 Gyr are also very consistent with AD measurements of stars in M31's disk, providing evidence that M31 may in fact have recently merged with a galaxy nearly 1/4 of its mass. Further work using high resolution zoom-in simulations is required to explore the contribution of internal heating to AD.