The two-point clustering of dark matter halos is influenced by halo properties besides mass, a phenomenon referred to as halo assembly bias. Using the depth of the gravitational potential well, V max , as our secondary halo property, in this paper we present the first study of the scale-dependence assembly bias. In the large-scale linear regime, r 10Mpc/h, our findings are in keeping with previous results. In particular, at the low-mass end (M vir < M coll ≈ 10 12.5 M /h), halos with high-V max show stronger large-scale clustering relative to halos with low-V max of the same mass; this trend weakens and reverses for M vir M coll . In the nonlinear regime, assembly bias in low-mass halos exhibits a pronounced scale-dependent "bump" at 500kpc/h − 5Mpc/h, a new result. This feature weakens and eventually vanishes for halos of higher mass. We show that this scale-dependent signature can primarily be attributed to a special subpopulation of ejected halos, defined as present-day host halos that were previously members of a higher-mass halo at some point in their past history. A corollary of our results is that galaxy clustering on scales of r ∼ 1 − 2Mpc/h can be impacted by up to ∼ 15% by the choice of the halo property used in the halo model, even for stellar mass-limited samples.