  We present ALMA observations of the Class I source Oph IRS63 in the context
of the Early Planet Formation in Embedded Disks (eDisk) large program. Our ALMA
observations of Oph IRS63 show a myriad of protostellar features, such as a
shell-like bipolar outflow (in $^{12}$CO), an extended rotating envelope
structure (in $^{13}$CO), a streamer connecting the envelope to the disk (in
C$^{18}$O), and several small-scale spiral structures seen towards the edge of
the dust continuum (in SO). By analyzing the velocity pattern of $^{13}$CO and
C$^{18}$O, we measure a protostellar mass of $\rm M_\star = 0.5 \pm 0.2 $~$\rm
M_\odot$ and confirm the presence of a disk rotating at almost Keplerian
velocity that extends up to $\sim260$ au. These calculations also show that the
gaseous disk is about four times larger than the dust disk, which could
indicate dust evolution and radial drift. Furthermore, we model the C$^{18}$O
streamer and SO spiral structures as features originating from an infalling
rotating structure that continuously feeds the young protostellar disk. We
compute an envelope-to-disk mass infall rate of $\sim 10^{-6}$~$\rm M_\odot \,
yr^{-1}$ and compare it to the disk-to-star mass accretion rate of $\sim
10^{-8}$~$\rm M_\odot \, yr^{-1}$, from which we infer that the protostellar
disk is in a mass build-up phase. At the current mass infall rate, we speculate
that soon the disk will become too massive to be gravitationally stable.
