  Context. Dynamically linking a meteor shower with its parent body is
challenging, and chaos in the dynamics of meteoroid streams may be one of the
reasons. For a robust identification of parent bodies, it is therefore
necessary to quantify the amount of chaos involved in the evolution of
meteoroid streams. Aims. The characterisation of chaos in meteoroid streams
thanks to chaos maps is still a new field of study. We aim to study two very
different meteoroid streams, the Draconids and the Leonids, in order to obtain
a general view of this topic. Methods. We use the method developed in a
previous paper dedicated to Geminids, drawing chaos maps with the orthogonal
fast Lyapunov indicator. We choose four particle size ranges to investigate the
effect of non-gravitational forces. As the dynamics is structured by
mean-motion resonances with planets, we compute the locations and widths of the
resonances at play. We use semi-analytical formulas valid for any eccentricity
and inclination and an arbitrary number of planets. Results. We pinpoint which
mean-motion resonances with Jupiter play a major role in the dynamics of each
meteoroid stream. We show how those resonances tend to trap mostly large
particles, preventing them from meeting with Jupiter. We also study particles
managing to escape those resonances, thanks to the gravitational perturbation
of Saturn for example. Finally, we explain why non-gravitational forces do not
disturb the dynamics much, contrary to what is observed for the Geminids.
