  In this article we revise the problem of anomalous values of pulsars' braking
indices n_{obs} and frequency second derivatives F2 arising in observations.
The intrinsic evolutionary braking is buried deep under superimposed irregular
processes, that prevent direct estimations of its parameters for the majority
of pulsars. We re-analyze the distribution of "ordinary" radio pulsars on a
F2-F1, F2-F0, F1-F0 and n_{obs}-tau_{ch} diagrams assuming their spin-down to
be the superposition of a "true" monotonous term and a symmetric oscillatory
term. We demonstrate that their effects may be clearly separated using simple
ad hoc arguments. Using maximum likelihood estimator we derive the parameters
of both components. We find characteristic timescales of such oscillations to
be of the order of 1e3-1e4 years, while its amplitudes are large enough to
modulate the observed spin-down rate up to 0.5-5 times and completely dominate
the second frequency derivatives. On the other hand, pulsars' secular evolution
is consistent with classical magnetodipolar model with braking index n ~ 3. So,
observed pulsars' characteristic ages (and similar estimators that depend on
the observed F1) are also affected by long term cyclic process and differ up to
0.5-5 times from their monotonous values. This fact naturally resolves the
discrepancy of characteristic and independently estimated physical ages of
several objects, as well as explains very large, up to 1e8 years,
characteristic ages of some pulsars. We discuss the possible physical
connection of long term oscillation with a complex neutron star rotation
relative its magnetic axis due to influence of the near-field part of
magnetodipolar torque.
