  The $\gamma$-ray emission from the W51 complex is widely acknowledged to be
attributed to the interaction between the cosmic rays (CRs) accelerated by the
shock of supernova remnant (SNR) W51C and the dense molecular clouds in the
adjacent star-forming region, W51B. However, the maximum acceleration
capability of W51C for CRs remains elusive. Based on observations conducted
with the Large High Altitude Air Shower Observatory (LHAASO), we report a
significant detection of $\gamma$ rays emanating from the W51 complex, with
energies from 2 TeV to 200 TeV. The LHAASO measurements, for the first time,
extend the $\gamma$-ray emission from the W51 complex beyond 100 TeV and reveal
a significant spectrum bending at tens of TeV. By combining the ``$\pi^0$-decay
bump" featured data from Fermi-LAT, the broadband $\gamma$-ray spectrum of the
W51 region can be well-characterized by a simple pp-collision model. The
observed spectral bending feature suggests an exponential cutoff at
$\sim400$~TeV or a power-law break at $\sim200$~TeV in the CR proton spectrum,
most likely providing the first evidence of SNRs serving as CR accelerators
approaching the PeV regime. Additionally, two young star clusters within W51B
could also be theoretically viable to produce the most energetic $\gamma$ rays
observed by LHAASO. Our findings strongly support the presence of extreme CR
accelerators within the W51 complex and provide new insights into the origin of
Galactic CRs.
