  The Large High Altitude Air Shower Observatory has reported the detection of
cosmic-ray sources in Milky Way that can accelerate particles up to PeV (=
10$^{15}$ eV) energies. These sources, so called ``PeVatrons'', are mostly
unidentified. Several classes of sources, such as supernova remnants, pulsar
wind nebula, or young stellar clusters can potentially be the counterparts of
these PeVatrons. The aim of this work is to study a pulsar wind nebula
interpretation of one of these PeVatrons, LHAASO J2226+6057, which has a
relatively well covered multi-frequency spectrum. We have performed a leptonic,
time-dependent modeling of the pulsar wind nebula (PWN) associated with PSR
J2229+6114 considering a time-energy-dependent diffusion-loss equation.
Injection, energy losses, as well as escape of particles were considered to
balance the time-dependent lepton population. We have also included the
dynamics of the PWN and the associated supernova remnant (SNR) and their
interaction via the reverse shock to study the reverberation phase of the
system. We have considered different values of braking index ($n$) and true age
($t_{age}$) for the fitting of the multi-wavelength (MWL) spectral energy
distribution (SED) of LHAASO J2226+6057. The best-fit PWN model parameters and
their 1$\sigma$ confidence intervals were evaluated. We have also demonstrated
the impact of reverberation on the MWL SED with increasing time. Additionally,
we have discussed the resultant large radius and low magnetic field associated
with the PWN in question, as caveats for the possible physical connection of
the pulsar as the origin of this high energy source.
