Four scenarios of disk evolution. (A) With M_* = 1 M_⊙, B_* = 0.44 kG, and P_* = 3 days, ${\dot{M}}_{\text{acc}}$ exceeds ${\dot{M}}_{\text{crit}}$ at 2.3 Myr, R_mag retreats inside R_cor, an IDW ceases, and stellar X-rays open a disk gap. (B) In the case of a more rapidly rotating (P_* = 2 days) star with a stronger (0.6 kG) field, ${\dot{M}}_{\text{acc}}$ never exceeds ${\dot{M}}_{\text{crit}}$ and no gap opens. (C) For a more slowly rotating (P_* = 7 day) star, there is no IDW but lower L_X and PE delays t_gap to 5.7 Myr. (D) In the 0.3 M_⊙ case, lower ${\dot{M}}_{\text{acc}}$ remains below ${\dot{M}}_{\text{crit}}$ for longer, delaying t_gap to 13.3 Myr.