  The magnetic interaction between a classical T Tauri star and its surrounding
accretion disk is thought to influence its rotational evolution. We use 2.5D
magnetohydrodynamic, axisymmetric simulations of star-disk interaction,
computed via the PLUTO code, to calculate the net torque acting on these stars.
We divide the net torque into three contributions: accretion (spin-up), stellar
winds (spin-down), and magnetospheric ejections (MEs) (spin-up or down). In
Paper I, we explored interaction regimes in which the stellar magnetosphere
truncates the inner disk at a location spinning faster than the star, resulting
in a strong net spin-up contribution from accretion and MEs ("steady accretion"
regime). In this paper, we investigate interaction regimes in which the
truncation radius gets closer to and even exceeds corotation, where it is
possible for the disk material to gain angular momentum and be periodically
ejected by the centrifugal barrier ("propeller" regime). This reduces the
accretion torque, can change the sign of the ME torque, and can result in a net
stellar spin-down configuration. These results suggest it is possible to have a
net spin-down stellar torque even for truncation radii within the corotation
radius ($R_\text{t} \gtrsim 0.7 R_\text{co}$). We fit semi-analytic functions
for the truncation radius, and the torque associated with star-disk interaction
(i.e., the sum of accretion and ME torques) and stellar wind, allowing for the
prediction of the net stellar torque for a parameter regime covering both net
spin-up and spin-down configurations, as well as the possibility of
investigating rotational evolution via 1D stellar evolution codes.
