  Gamma-ray bursts (GRBs) 201015A and 201216C are valuable cases with detection
of very high energy (VHE) gamma-ray afterglows. By analysing their prompt
emission data, we find that GRB 201216C is an extremely energetic long GRB with
a hard gamma-ray spectrum, while GRB 201015A is a relative sub-energetic, soft
spectrum GRB. Attributing their radio-optical-X-ray afterglows to the
synchrotron radiation of the relativistic electrons accelerated in their jets,
we fit their afterglow lightcurves with the standard external shock model and
infer their VHE afterglows from the synchrotron self-Compton scattering process
of the electrons. It is found that the jet of GRB 201015A is mid-relativistic
($\Gamma_0=44$) surrounded by a very dense medium ($n=1202$ cm$^{-3}$) and the
jet of GRB 201216C is ultra-relativistic ($\Gamma_0=331$) surrounded by a
moderate dense medium ($n=5$ cm$^{-3}$). The inferred peak luminosity of the
VHE gamma-ray afterglows of GRB 201216C is approximately $10^{-9}$ erg
cm$^{-2}$ s$^{-1}$ at $57-600$ seconds after the GRB trigger, making it can be
detectable with the MAGIC telescopes at a high confidence level, even the GRB
is at a redshift of 1.1. Comparing their intrinsic VHE gamma-ray lightcurves
and spectral energy distributions with GRBs~180720B, 190114C, and 190829A, we
show that their intrinsic peak luminosity of VHE gamma-ray afterglows at
$10^{4}$ seconds post the GRB trigger is variable from $10^{45}$ to $5\times
10^{48}$ erg s$^{-1}$, and their kinetic energy, initial Lorentz factor, and
medium density are diverse among bursts.
