  We present a large-scale study of stellar rotation for T Tauri stars in the
Orion Star-Forming Complex. We use the projected rotational velocity
($v\sin(i)$) estimations reported by the APOGEE-2 collaboration as well as
individual masses and ages derived from the position of the stars in the HR
diagram, considering Gaia-EDR3 parallaxes and photometry plus diverse
evolutionary models. We find an empirical trend for $v\sin(i)$ decreasing with
age for low-mass stars ($0.4 M_{\odot} < M_{\ast} < 1.2 M_{\odot}$). Our
results support the existence of a mechanism linking $v\sin(i)$ to the presence
of accreting protoplanetary disks, responsible for regulating stellar rotation
in timescales of about 6 Myr, which is the timescale in which most of the T
Tauri stars lose their inner disk. Our results provide important constraints to
models of rotation in the early phases of evolution of young stars and their
disks.
