  Constraining the physical and chemical structure of young embedded disks is
crucial to understanding the earliest stages of planet formation. As part of
the Early Planet Formation in Embedded Disks Atacama Large
Millimeter/submillimeter Array Large Program, we present high spatial
resolution ($\sim$0$.\!\!^{\prime\prime}$1 or $\sim$15 au) observations of the
1.3 mm continuum and $^{13}$CO $J=$ 2-1, C$^{18}$O $J=$ 2-1, and SO $J_N=$
$6_5$-$5_4$ molecular lines toward the disk around the Class I protostar L1489
IRS. The continuum emission shows a ring-like structure at 56 au from the
central protostar and a tenuous, optically thin emission extending beyond
$\sim$300 au. The $^{13}$CO emission traces the warm disk surface, while the
C$^{18}$O emission originates from near the disk midplane. The coincidence of
the radial emission peak of C$^{18}$O with the dust ring may indicate a
gap-ring structure in the gaseous disk as well. The SO emission shows a highly
complex distribution, including a compact, prominent component at $\lesssim$30
au, which is likely to originate from thermally sublimated SO molecules. The
compact SO emission also shows a velocity gradient along a slightly
($\sim15^\circ$) tilted direction with respect to the major axis of the dust
disk, which we interpret as an inner warped disk in addition to the warp around
$\sim$200 au suggested by previous work. These warped structures may be formed
by a planet or companion with an inclined orbit, or by a gradual change in the
angular momentum axis during gas infall.
