  Understanding how material accretes onto the rotationally supported disk from
the surrounding envelope of gas and dust in the youngest protostellar systems
is important for describing how disks are formed. Magnetohydrodynamic
simulations of magnetized, turbulent disk formation usually show spiral-like
streams of material (accretion flows) connecting the envelope to the disk.
However, accretion flows in these early stages of protostellar formation still
remain poorly characterized due to their low intensity and possibly some
extended structures are disregarded as being part of the outflow cavity. We use
ALMA archival data of a young Class 0 protostar, Lupus 3-MMS, to uncover four
extended accretion flow-like structures in C$^{18}$O that follow the edges of
the outflows. We make various types of position-velocity cuts to compare with
the outflows and find the extended structures are not consistent with the
outflow emission, but rather more consistent with a simple infall model. We
then use a dendrogram algorithm to isolate five sub-structures in
position-position-velocity space. Four out of the five sub-structures fit well
($>$95%) with our simple infall model, with specific angular momenta between
$2.7-6.9\times10^{-4}\,$km$\,$s$^{-1}\,$pc and mass-infall rates of
$0.5-1.1\times10^{-6}\,M_{\odot}\,$yr$^{-1}$. Better characterization of the
physical structure in the supposed "outflow-cavities" is important to
disentangle the true outflow cavities and accretion flows.
