We investigate how the stellar rotational support changes as a function of spatially resolved stellar population age (D(n)4000) and relative central stellar surface density (Delta Sigma(1)) for MaNGA isolated/central disc galaxies. We find that the galaxy rotational support indicator lambda(Re) varies smoothly as a function of Delta Sigma(1) and D(n)4000. D(n)4000 versus Delta Sigma 1 follows a 'J-shape', with lambda(Re) contributing to the scatters. In this 'J-shaped' pattern rotational support increases with central D(n)4000 when Delta Sigma(1) is low but decreases with Delta Sigma(1) when Delta Sigma(1) is high. Restricting attention to low-Delta Sigma(1) (i.e. large-radius) galaxies, we suggest that the trend of increasing rotational support with D(n)4000 for these objects is produced by a mix of two different processes, a primary trend characterized by growth in lambda Re along with mass through gas accretion, on top of which disturbance episodes are overlaid, which reduce rotational support and trigger increased star formation. An additional finding is that star-forming galaxies with low Delta Sigma(1) have relatively larger radii than galaxies with higher Delta Sigma(1) at fixed stellar mass. Assuming that these relative radii rankings are preserved while galaxies are star forming then implies clear evolutionary paths in central D(n)4000 versus Delta Sigma(1). The paper closes with comments on the implications that these paths have for the evolution of pseudo-bulges versus classical bulges. The utility of using D(n)4000-Delta Sigma(1) to study lambda(Re) reinforces the notion that galaxy kinematics correlate both with structure and with stellar-population state, and indicates the importance of a multidimensional description for understanding bulge and galaxy evolution.