  We present deep Very Large Array imaging of 3C~273 in order to determine the
diffuse, large scale radio structure of this famous radio-loud quasar. Diffuse
extended structure (radio lobes) is detected for the first time in these
observations as a consequence of high dynamic range in the 327.5 and 1365 MHz
images. This emission is used to estimate a time averaged jet power, $7.2
\times 10^{43} \rm{~ergs~s^{-1}} < \overline{Q} < 3.7 \times 10^{44}
\rm{~ergs~s^{-1}}$. Brightness temperature arguments indicate consistent values
of the time variability Doppler factor and the compactness Doppler factor for
the inner jet, $\delta \gtrsim 10$. Thus, the large apparent broadband
bolometric luminosity of the jet, $\sim 3 \times 10^{46}\rm{~ergs~s^{-1}}$,
corresponds to a modest intrinsic luminosity $\gtrsim
10^{42}\rm{~ergs~s^{-1}}$, or $\sim 1\%$ of $\overline{Q}$. In summary, we find
that 3C~273 is actually a "typical" radio loud quasar contrary to suggestions
in the literature. The modest $\overline{Q}$ is near the peak of the luminosity
distribution for radio loud quasars and it is consistent with the current rate
of dissipation emitted from millimeter wavelengths to gamma rays. The extreme
core-jet morphology is an illusion from a near pole-on line of sight to a
highly relativistic jet that produces a Doppler enhanced glow that previously
swamped the lobe emission. 3C~273 apparently has the intrinsic kpc scale
morphology of a classical double radio source, but it is distorted by an
extreme Doppler aberration.
