The beta Cephei star delta Ceti was considered one of the few monoperiodic variables in its class. Despite ( or perhaps because of) its apparently simple oscillation spectrum, it has been challenging and controversial to identify this star's pulsation mode and constrain its physical parameters seismically. Broadband time-resolved photometry of delta Ceti spanning 18.7 days with a duty cycle of about 65% obtained by the Microvariability and Oscillations of Stars ( MOST) satellite-the first scientific observations ever obtained by MOST-reveals that the star is actually multiperiodic. Besides the well-known dominant frequency of f(1) = 6.205886 day(-1), we have discovered in the MOST data its first harmonic 2f(1) and three other frequencies (f(2) 3.737, f(3) 3.673, and f(4) = 0.318 day(-1)), all detected with a signal-to-noise ratio (S/N) > 4. In retrospect, f(2) was also present in archival spectral line-profile data but at lower S/N. We present seismic models whose modes match exactly the frequencies f1 and f2. Only one model falls within the common part of the error boxes of the star's observed surface gravity and effective temperature from photometry and spectroscopy. In this model, f1 is the radial (l = 0) first overtone, and f(2) is the g(2) (l = 2, m = 0) mode. This model has a mass of 10.2 +/- 0.2 M-circle dot and an age of 17.9 +/- 0: 3 Myr, making delta Ceti an evolved beta Cephei star. If f(2) and f(3) are rotationally split components of the same g2 mode, then the star's equatorial rotation velocity is either 27.6 km s(-1) or half this value. Given its v sin i of about 1 km s(-1), this implies that we are seeing delta Ceti nearly pole-on.