  We present ALMA Band-3/7 observations towards "the Heart" of a massive
hub-filament system (HFS) SDC335, to investigate its fragmentation and
accretion. At a resolution of $\sim0.03$ pc, 3 mm continuum emission resolves
two massive dense cores MM1 and MM2, with $383(^{+234}_{-120})$ $M_\odot$
(10-24% mass of "the Heart") and $74(^{+47}_{-24})$ $M_\odot$, respectively.
With a resolution down to 0.01 pc, 0.87 mm continuum emission shows MM1 further
fragments into six condensations and multi-transition lines of H$_2$CS provide
temperature estimation. The relation between separation and mass of
condensations at a scale of 0.01 pc favors turbulent Jeans fragmentation where
the turbulence seems to be scale-free rather than scale-dependent. We use the
H$^{13}$CO$^+$ (1-0) emission line to resolve the complex gas motion inside
"the Heart" in position-position-velocity space. We identify four major gas
streams connected to large-scale filaments, inheriting the anti-clockwise
spiral pattern. Along these streams, gas feeds the central massive core MM1.
Assuming an inclination angle of $45(\pm15)^{\circ}$ and a H$^{13}$CO$^+$
abundance of $5(\pm3)\times10^{-11}$, the total mass infall rate is estimated
to be $2.40(\pm0.78)\times10^{-3}$ $M_\odot$ yr$^{-1}$, numerically consistent
with the accretion rates derived from the clump-scale spherical infall model
and the core-scale outflows. The consistency suggests a continuous, near
steady-state, and efficient accretion from global collapse, therefore ensuring
core feeding. Our comprehensive study of SDC335 showcases the detailed gas
kinematics in a prototypical massive infalling clump and calls for further
systematic and statistical analyses in a large sample.
