  We present 1.3 mm observations of the Sun-like star $\tau$ Ceti with the
Atacama Large Millimeter/submillimeter Array (ALMA) that probe angular scales
of $\sim1$'' (4 AU). This first interferometric image of the $\tau$ Ceti
system, which hosts both a debris disk and possible multiplanet system, shows
emission from a nearly face-on belt of cold dust with a position angle of
$90^\circ$ surrounding an unresolved central source at the stellar position. To
characterize this emission structure, we fit parametric models to the
millimeter visibilities. The resulting best-fit model yields an inner belt edge
of $6.2^{+9.8}_{-4.6}$ AU, consistent with inferences from lower resolution,
far-infrared Herschel observations. While the limited data at sufficiently
short baselines preclude us from placing stronger constraints on the belt
properties and its relation to the proposed five planet system, the
observations do provide a strong lower limit on the fractional width of the
belt, $\Delta R/R > 0.75$ with $99\%$ confidence. This fractional width is more
similar to broad disks such as HD 107146 than narrow belts such as the Kuiper
Belt and Fomalhaut. The unresolved central source has a higher flux density
than the predicted flux of the stellar photosphere at 1.3 mm. Given previous
measurements of an excess by a factor of $\sim2$ at 8.7 mm, this emission is
likely due to a hot stellar chromosphere.
