Observations of young, embedded disks are essential for understanding the early stages of planet formation. As part of the Early Planet Formation in Embedded Disks (eDisk) ALMA Large Program, we present high angular resolution (~15 au) observations of the 1.3 mm continuum and CO isotopologue and SO molecular line emission toward the disk around the Class I protostar L1489 IRS. While the <sup>13</sup>CO (<i>J</i> = 2?1) emission originates from the warm disk surface, the dust continuum emission and the C<sup>18</sup>O (<i>J</i> = 2?1) emission trace near the disk midplane and show a ring-like structure at ~56 au radius. The SO (<i>J<sub>N</sub></i> = 6<sub>5</sub>?5<sub>4</sub>) emission shows a complex distribution. While a diffuse emission is seen in the outer region (> 200 au), a compact, prominent component is observed in the innermost region (< 30 au). The compact SO emission shows a velocity gradient along a slightly (~15 deg) tilted direction with respect to the dusty disk, suggesting a warped structure at ~30 au in addition to another disk warp at ~200 au reported in a previous study. These ringed and warped structures could be explained by a planet or companion with an inclined orbit, or by a gradual change in the direction of the angular momentum axis during gas infall. Our observations reveal potential planet formation in a highly dynamic environment of young Class I disks.