  We revisit the issue of period variation of the recently claimed red nova
precursor candidate KIC 9832227. By using the data gathered during the main
mission of the Kepler satellite, those collected by ground-based wide-field
surveys and other monitoring programs (such as ASAS-SN), we find that the
currently available timing data strongly support a model consisting of the
known W UMa binary and a distant low-mass companion with an orbital period of
~13.5 years. The period of the W UMa component exhibits a linear period
decrease with a pace of (1.10+/-0.05)x10^{-6} days per year, within the range
of many other similar systems. This rate of decrease is several orders of
magnitude lower than that of V1309 Sco, the first (and so far the only)
well-established binary precursor of a nova observed a few years before the
outburst. The high-fidelity fit of the timing data and the conformity of the
derived minimum mass of (0.38+/-0.02) Msun of the outer companion from these
data with the limit posed by the spectroscopic non-detection of this component,
are in agreement with the suggested hierarchical nature of this system.
