  We present the analysis of an eccentric, partially eclipsing long-period
($P=19.23$ d) binary system KIC 9777062 that contains main sequence stars near
the turnoff of the intermediate age open cluster NGC 6811. The primary is a
metal-lined Am star with a possible convective blueshift to its radial
velocities, and one star (probably the secondary) is likely to be a $\gamma$
Dor pulsator. The component masses are $1.603\pm0.006$(stat.)$\pm0.016$(sys.)
and $1.419\pm0.003\pm0.008 M_\odot$, and the radii are $1.744\pm0.004\pm0.002$
and $1.544\pm0.002\pm0.002 R_\odot$. The isochrone ages of the stars are mildly
inconsistent: the age from the mass-radius combination for the primary
($1.05\pm0.05\pm0.09$ Gyr, where the last quote was systematic uncertainty from
models and metallicity) is smaller than that from the secondary
($1.21\pm0.05\pm0.15$ Gyr) and is consistent with the inference from the
color-magnitude diagram ($1.00\pm0.05$ Gyr).
  We have improved the measurements of the asteroseismic parameters $\Delta
\nu$ and $\nu_{\rm max}$ for helium-burning stars in the cluster. The masses of
the stars appear to be larger (or alternately, the radii appear to be smaller)
than predicted from isochrones using the ages derived from the eclipsing stars.
  The majority of stars near the cluster turnoff are pulsating stars: we
identify a sample of 28 $\delta$ Sct, 15 $\gamma$ Dor, and 5 hybrid types. We
used the period-luminosity relation for high-amplitude $\delta$ Sct stars to
fit the ensemble of the strongest frequencies for the cluster members, finding
$(m-M)_V = 10.37\pm0.03$. This is larger than most previous determinations, but
smaller than values derived from the eclipsing binary ($10.47\pm0.05$).
