  Organic features lead to two distinct types of Class 0/I low-mass protostars:
hot corino sources, and warm carbon-chain chemistry (WCCC) sources. Some
observations suggest that the chemical variations between WCCC sources and hot
corino sources are associated with local environments, as well as the
luminosity of protostars. We conducted gas-grain chemical simulation in
collapsing protostellar cores, and found that the fiducial model predicts
abundant carbon-chain molecules and COMs, and reproduces WCCC and hot corino
chemistry in the hybrid source L483. By changing values of some physical
parameters, including the visual extinction of ambient clouds ($A_{\rm V}^{\rm
amb}$), the cosmic-ray ionization rate ($\zeta$), the maximum temperature
during the warm-up phase ($T_{\rm max}$), and the contraction timescale of
protostars ($t_{\rm cont}$), we found that UV photons and cosmic rays can boost
WCCC features by accelerating the dissociation of CO and CH$_4$ molecules. On
the other hand, UV photons can weaken the hot corino chemistry by
photodissociation reactions, while the dependence of hot corino chemistry on
cosmic rays is relatively complex. The $T_{\rm max}$ does not affect WCCC
features, while it can influence hot corino chemistry by changing the effective
duration of two-body surface reactions for most COMs. The long $t_{\rm cont}$
can boost WCCC and hot corino chemistry, by prolonging the effective duration
of WCCC reactions in the gas phase and surface formation reactions for COMs,
respectively. Subsequently, we ran a model with different physical parameters
to reproduce scarce COMs in prototypical WCCC sources. The scarcity of COMs in
prototypical WCCC sources can be explained by insufficient dust temperature in
the inner envelopes to activate hot corino chemistry. Meanwhile, the High
$\zeta$ and the long $t_{\rm cont}$ favors the explanation for scarce COMs in
these sources.
