<jats:title>ABSTRACT</jats:title> <jats:p>Using Keck/NIRC2 <jats:inline-formula> <jats:tex-math> <?CDATA ${L}^{\prime }$?> </jats:tex-math> <?MML <mml:math> <mml:msup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mo accent="true">′</mml:mo> </mml:mrow> </mml:msup> </mml:math>?> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjl522776ieqn1.gif" xlink:type="simple" /> </jats:inline-formula> (3.78 <jats:italic>μ</jats:italic>m) data, we report the direct imaging discovery of a scattered-light-resolved, solar-system-scale residual protoplanetary disk around the young A-type star HD 141569A, interior to and concentric with the two ring-like structures at wider separations. The disk is resolved down to ∼0.″25 and appears as an arc-like rim with attached hook-like features. It is located at an angular separation intermediate between that of warm CO gas identified from spatially resolved mid-infrared spectroscopy and diffuse dust emission recently discovered with the <jats:italic>Hubble Space Telescope</jats:italic>. The inner disk has a radius of ∼39 au, a position angle consistent with north up, and an inclination of <jats:italic>i</jats:italic> ∼ 56<jats:sup>o</jats:sup> and has a center offset from the star. Forward modeling of the disk favors a thick torus-like emission sharply truncated at separations beyond the torus’s photocenter and heavily depleted at smaller separations. In particular, the best-fit density power law for the dust suggests that the inner disk dust and gas (as probed by CO) are radially segregated, a feature consistent with the dust trapping mechanism inferred from observations of “canonical” transitional disks. However, the inner disk component may instead be explained by radiation pressure-induced migration in optically thin conditions, in contrast to the two stellar companion/planet-influenced ring-like structures at wider separations. HD 141569A’s circumstellar environment—with three nested, gapped, concentric dust populations—is an excellent laboratory for understanding the relationship between planet formation and the evolution of both dust grains and disk architecture.</jats:p>