  We present a comprehensive investigation on the mass function (MF) of a
snake-like stellar structure in the solar neighbourhood, building on our
previous discovery. To ensure the reliability of the data, we reselect the
member stars of the Stellar ``Snake'' in the latest {\it Gaia} Data Release 3
using the same approach as the initial series of articles. We also precisely
measure the physical parameters of the clusters within the Stellar Snake. In
light of the high completeness of the member stars in the cluster regions, we
develop a simulated model color-magnitude diagram-based inference method to
derive the mass function, binary fraction, and mass-ratio distribution of the
clusters in the Stellar Snake. Notably, despite their similar ages and
metallicity, we discover systematic variations in the MFs along the elongation
direction of the Snake in the mass range of 0.5 to 2.0 M$_\odot$. The ``head''
of the Snake conforms to a canonical initial mass function with a power-law
slope of $\alpha\sim-2.3$. Extending towards the ``tail,'' the MF becomes more
top-light, indicating a deficiency of massive stars within these clusters. This
result provides evidence for the delayed formation of massive stars in the
clusters. Such clues give support to the hypothesis that the Stellar Snake
constitutes as a hierarchically primordial structure.
