[en] We investigate the propagation of ∼0.3-300 keV electrons in five solar impulsive electron events, observed by the WIND three-dimensional Plasma and Energetic Particle instrument, that have rapid-rise and rapid-decay temporal profiles. In two events, the temporal profiles above 25 keV show a second peak of inward-traveling electrons tens of minutes after the first peak, followed by a third peak due to outward-traveling electrons minutes later-likely due to reflection/scattering first at ∼0.7-1.7 AU past the Earth, and then in the inner heliosphere inside 1 AU. In the five events, below a transition energy E₀ (∼10-40 keV), the pitch-angle distributions are highly anisotropic with a pitch-angle width at half-maximum (PAHM) of <15⁰ (unresolved) through the time of the peak; the ratio Λ of the peak flux of scattered (22.⁰5-90⁰ relative to the outward direction) to field-aligned scatter-free (0⁰-22.⁰5) electrons is ∼<0.1. Above E₀, the PAHM at the flux peak increases with energy up to 85⁰ at 300 keV, and Λ also increases with energy up to ∼0.8 at 300 keV. Thus, low-energy electrons propagated essentially scatter-free through the interplanetary medium, while high-energy electrons experienced pitch-angle scattering, with scattering strength increasing with energy. The transition energy E₀ between the two populations is always such that the electron gyroradius (ρ_e) is approximately equal to the local thermal proton gyroradius (ρ_Tp), suggesting that the higher energy electrons were scattered by resonance with turbulent fluctuations at scale ∼>ρ_Tp in the solar wind.