  In the standard cosmological model the dark energy (DE) and nonrelativistic
(NR) matter densities are observationally determined to be comparable at the
present time, in spite of their greatly different evolution histories. This
`cosmic coincidence' enigma -- also referred to as the `why now? problem' --
relies, by its very definition, on the implicit prior expectation for our
`typicality' in the cosmic (expanding) spacetime volume. Otherwise, this
conundrum does not exist in the first place. It is shown here that this
apparent coincidence could be explained as a non-anthropic observational
selection effect: for us to be typical observers in the comoving (static)
spacetime volume, the cosmic energy budget must contain a non-vanishing DE
component. In addition, it is shown that irrespective of the cosmological
initial conditions and assuming no `new physics', the Universe is most likely
to be observed at a time when the conformal Hubble radius, $\mathcal{H}^{-1}$,
attains a maximum. The latter takes place at the epoch when $\rho_{DE}$ and
$\rho_{m}$, the energy densities of DE and NR matter, respectively, are
comparable. Specifically, our presumed `typicality' along the conformal
timeline, coupled to a few other plausible assumptions, implies that
$R\equiv\rho_{DE}/\rho_{m}$ is `sampled' from a Beta Prime probability
distribution function. A priori 68\% (95\%) confidence range for the ratio is
$0.20<R<3.46$ ($0.033<R<17.20$), with an expectation value of $\bar{R}=3.5$.
These are in agreement with the observationally inferred value, $R_{obs}=2.23$.
