  Using data from the HAWC gamma-ray Telescope, we have studied a sample of 37
millisecond pulsars (MSPs), selected for their spindown power and proximity.
From among these MSP, we have identified four which favor the presence of very
high-energy gamma-ray emission at a level of $(2\Delta \ln \mathcal{L})^{1/2}
\ge 2.5$. Adopting a correlation between the spindown power and gamma-ray
luminosity of each pulsar, we performed a stacked likelihood analysis of these
37 MSPs, finding that the data supports the conclusion that these sources emit
very high-energy gamma-rays at a level of $(2\Delta \ln \mathcal{L})^{1/2} =
4.24$. Among sets of randomly selected sky locations within HAWC's
field-of-view, less than 1\% of such realizations yielded such high statistical
significance. Our analysis suggests that MSPs produce very high-energy
gamma-ray emission with a similar efficiency to that observed from the Geminga
TeV-halo, $\eta_{\rm MSP} = (0.39-1.08) \times \eta_{\rm Geminga}$. This
conclusion poses a significant challenge for pulsar interpretations of the
Galactic Center gamma-ray excess, as it suggests that any population of MSPs
potentially capable of producing the GeV excess would also produce TeV-scale
emission in excess of that observed by HESS from this region. Future
observations by CTA will be able to substantially clarify this situation.
